NOAA/NGDC candidate models for the 11th generation International Geomagnetic Reference Field and the concurrent release of the 6th generation Pomme magnetic model
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The International Geomagnetic Reference Field (IGRF) is updated every five years based on candidate model submissions by research institutions worldwide. In the call for the 11th generation of IGRF, candidates were requested for the definitive main field in 2005, the predicted main field in 2010, and the predicted secular variation from 2010 to 2015. The NOAA/NGDC candidate models for IGRF-11 were produced from parent models parameterized in the same way as the 6th generation of our Pomme magnetic model. All models were based on CHAMP satellite measurements, while Ørsted satellite measurements were used for model validation. The internal field in Pomme-6 is described by a 2nd degree Taylor time series of spherical harmonic expansion coefficients of a scalar magnetic potential. Magnetic fields of ionospheric origin are avoided by careful data selection. Instead of co-estimating magnetospheric fields, we subtract a magnetospheric field model estimated previously from a more extensive data set covering all local times. From comparison with Ørsted measurements and general considerations of magnetic field predictability, we attribute a root mean square (RMS) uncertainty of 1.3 nT to our candidate model for the main field in 2005, 2.5 nT to the predicted main field in 2010 and 26 nT/a to the predicted secular variation from 2010 to 2015.
Key wordsMagnetic field magnetic satellite magnetic reference field main field magnetic field modeling
Models of the geomagnetic main field enjoy widespread use in navigation and pointing devices. They also provide essential information on the geometry and strength of the geomagnetic field for models of the ionosphere and magnetosphere, used for example in space weather forecasting. The preferred model for engineering applications is the World Magnetic Model, WMM (Maus et al., 2010), a degree and order 12 model with fixed format, guaranteed support and release date. The preferred model of the scientific community is the International Geomagnetic Reference Field, IGRF (e.g. Maus et al., 2005), produced in an international collaborative effort under the leadership of the International Association for Geomagnetism and Aeronomy. The degree and precision of the IGRF has changed over time reflecting the increased accuracy of the underlying observing systems. While the WMM is a purely predictive model, the IGRF is adjusted retrospectively to provide more accurate “definitive” models for past epochs. In the year preceding the new 5-year epoch, a call is issued for candidates for the definitive main field at the end of the previous epoch (in this case 2005.0), a predictive main field model for the upcoming start of the new epoch (2010.0), and the predicted temporal change (secular variation) over the upcoming epoch (2010.0–2015.0). Here we describe our respective candidates and the parent models from which these were derived.
Since the IGRF only describes the long-wavelength internal part of the geomagnetic field, candidate models are usually extracted from more extensive models which include higher-degree contributions of the internal field, second-degree temporal derivatives (secular acceleration) and simple parameterizations of external fields of magnetospheric origins. Recent examples include the Pomme magnetic model (Maus et al., 2006), the CHAMP, Ørsted and SAC-C based CHAOS model (Olsen et al., 2006) and the GFZ Reference Internal Magnetic Model, GRIMM (Lesur et al., 2008). Such more sophisticated main field models are widely used in geomagnetism for studies of the dynamics of the earth’s core (e.g. Hulot et al., 2002). Particularly accurate main field models are also required in the calibration of space-borne magnetometers, such as on the Communication and Navigation Outage Forecast Satellite C/NOFS (De La Beaujardiere, 2004).
Researchers deriving models of the main geomagnetic field can use a wide range of magnetic measurements including the network of magnetic observatories and the three satellite magnetic missions Ørsted (1999, ongoing), CHAMP (2000, ongoing) and SAC-C (2000–2004) (e.g. Lühr et al., 2009). Of the three satellites, CHAMP (Reigber et al., 2002) arguably provides the optimal data basis, with close to 100% data retrieval rate, small polar gap and dual-head star camera for low-noise attitude determination. We therefore base our main field models presented here entirely on CHAMP measurements and using Ørsted vector and scalar measurements for independent validation.
2. Data Selection, Processing and Model Estimation
2.1 Data selection
Due to the well-known spatial aliasing and crustal bias problems with ground-based observatory data, only satellite data were used in the actual model estimation. However, ground-based observatory data played an important role in data selection by providing the source of the Dst and am indices.
The candidate models were entirely based on data from the CHAMP satellite. Ørsted data were processed simultaneously and used for validation of the processing steps and parent models. Ørsted data were also used in estimating the uncertainties of the Gauss coefficients.
All satellite data were sub-sampled to 20 seconds, corresponding to about 150 km along-track spacing. Separate data sets were compiled for mid latitudes (−60° to 60° geomagnetic latitude) and high latitudes (>50° and <−50° geomagnetic latitude). Vector data were only used at mid latitudes. Scalar and vector data at mid latitudes were selected from the 22:00–5:00 local time sector for CHAMP and 20:00–5:00 LT for Ørsted.
CHAMP data prior to 22:00 were excluded due to the disturbing diamagnetic effect of the ambient plasma. This effect is insignificant at Ørsted altitude. Data at high latitudes were used from all local times. No exclusion for certain solar zenith angle ranges was made, since this would lead to decimated track segments. Such shortened track segments would make it difficult to compare the root mean square (RMS) residuals of neighboring tracks (see below). Specifically for CHAMP data we demanded that attitude data from dual-head star camera mode and electron density and temperature measurements were available.
In a final data selection step, the RMS values of along-track residuals against Pomme-5 (http://geomag.org/models/Pomme5.html) were sorted by longitude of the equator crossing and by date, separately for mid latitudes and for northern and southern high latitude track segments. Then the following test was carried out for each track: Its RMS value was compared with the mean RMS value of all neighboring tracks within an 8° longitude range and within a one year time bin. If it was found that this track had one neighbor to the east and another neighbor to the west with an RMS at least 3 nT smaller, then this track was declared as “noisy” and was eliminated from the data set. The threshold of 3 nT was found by trial and error to perform well at excluding noisy data while retaining good spatial data coverage. Thus, the absolute residuals against Pomme-5 were not a selection criterion. Instead, the relative agreement with Pomme-5, as compared with neighboring tracks, was used.
2.2 Data corrections and weighting
Estimated angular corrections for the misalignment between the magnetometer reference system and the star tracker reference system on the CHAMP satellite are used to correct the vector data accordingly.
The magnetic signals of motional induction in the oceans due to the 8 major tidal constituents up to spherical harmonic degree 45 are subtracted, as predicted by Kuvshinov and Olsen (2004).
The signature of plasma pressure gradient currents is subtracted using the correction for the “diamagnetic effect”, as proposed by Lühr et al. (2003), making use of actual electron density and temperature measurements by CHAMP.
A magnetospheric field model was subtracted from the data. Due to the local-time asymmetry of magnetospheric fields, day-side data have to be included in their modeling. Since day-side data are too noisy for being included in the modeling of the main field, the magnetospheric fields are best estimated in a separate precessing step. We used a revised version of the model described in Maus and Lühr (2005) which now includes the solar cycle dependence of the magnetospheric ring current. This 18-parameter model quantifies the quiet-time magnetospheric fields, modulated by the Interplanetary Magnetic Field and solar activity. Details of the model are described in Lühr and Maus (2010, this issue).
The local data density per unit area was determined, and data were then weighted accordingly in order to achieve approximate uniform spatial representation in the inversion.
2.3 Model descriptions
The static part of the internal field to degree and order 40 for the two parent models and to degree and order 60 for Pomme-6
The secular variation (SV) to degree and order 16
The secular acceleration (SA) to degree and order 16. For Pomme-6 separate coefficients of the SA are provided for the periods before and after the mid point of the data interval in 2005.0. This temporal representation with two sets of S A coefficients and a single set of SV coefficients was first introduced in Pomme-4 (http://geomag.org/models/pomme4.html).
A daily varying degree-1 external field, as proposed by Olsen et al. (2006), represented by a single value of the strength of the axial dipole in Solar-Magnetic, SM, frame for every 24 h interval.
The model coefficients were estimated in a non-iterative least-squares approach, where the information from the scalar data was linearized using Pomme-5. The SV was regularized starting at degree and order 14, while the SA coefficients were damped for degrees 9 and higher, as described in Maus et al. (2006).
For Pomme-6 the entire available CHAMP data were used from 2000.6 to 2009.7.
To estimate the main field in 2005.0, we chose satellite data from 2003.5 to 2006.5. The primary parent model was produced from CHAMP data only. A second parent model was produced by including Ørsted scalar data. This model was only used for validation and to estimate the uncertainty of the coefficients of the first model. For this purpose it would have been better to have a completely independent model of pure Ørsted data. However, since Ørsted stopped supplying vector measurements after 2003, it was not possible to produce an accurate model from Ørsted-only data.
To predict the main field in 2010.0 and the secular variation 2010–2015, we used the last three years of available data, spanning 2006.5–2009.7. Again, the primary parent model was based only on CHAMP data, while a second model including Ørsted data was used for estimating Gauss coefficient uncertainties.
2.4 Derivation of candidate model coefficients and uncertainties
The main field in 2005.0 was simply taken as the static coefficients at the center of the CHAMP-only model. Their uncertainty was estimated by taking the difference to the corresponding coefficients of the model including Ørsted data, and multiplying the difference by three. The ad-hoc rationale for the factor three is that the Ørsted data had 1/3 weight in the combined model, so a “pure” Ørsted model would presumably exhibit three times the observed deviation to the CHAMP-only model. A minimum uncertainty of 0.01 nT was imposed in order to reflect the added uncertainty due to rounding errors. The total RMS uncertainty in the vector field averaged over the Earth surface can be inferred from the square root of the total Lowes/Mauersberger power. It amounts to 1.3 nT.
The main field in 2010.0 was predicted by evaluating the Taylor time series using secular variation and secular acceleration coefficients for the date 2010.0. The uncertainties were evaluated in the same way as for the 2005 model. The total RMS uncertainty is estimated as 2.5 nT
Studies of fore- and hind-cast of the secular variation of the geomagnetic field (e.g. Maus et al., 2008) suggest that the predictive quality of the secular acceleration seems to be quite limited. Taking a pessimistic view, we therefore provide the SV of the parent model at the end of the data interval (2009.67) as our best estimate of the SV 2010–2015. The primary uncertainty in SV forecast lies in the unpredictable behavior of the SA. As an estimate of uncertainty combining measurement and prediction uncertainties, we therefore take the difference between the SV of the CHAMP model in 2009.67 and the forward-extrapolated SV (using the SA coefficients) of the combined model to 2012.5. The latter accounts for unpredictable changes in the true SV, in addition to the uncertainty in estimating the present SV. This approach leads to a large (but realistic) uncertainty estimate of 26 nT/a. This means that we expect the cumulative RMS error of the IGRF to reach 130 nT by the end of the model epoch in 2015.
2.5 Test models with extended-degree secular variation
Presently, the predictive secular variation of the IGRF only extends to degree and order 8, a relict of the presatellite era in which the high-degree SV was impossible to observe. With the present satellite coverage, it is possible to obtain an un-damped estimate of the SV to degree 13 from only 3 years of data. It therefore would have seemed obvious to extend the predictive SV from degree 8 to degree 13, already for the epoch 2005–2010. However, this suggestion was dismissed in 2004 and again in 2009, even though a study by Silva et al. (2010), this issue), presented at IAGA-2009 in Sopron, demonstrated that the SV coefficients at degrees 9–12 of the parent models for IGRF-2005 provided a significantly better estimate of the SV in the 2005–2010 epoch than the current practice of setting these SV coefficients to zero. In order to further strengthen the case for extending the predictive SV to degree 13 in 2014 for IGRF-12, all groups were asked to provide extended-degree test versions of their SV candidate models. These extended-degree test models can then be compared with the true SV in subsequent years in order to assess the reliability of high-degree SV predictions.
The extended-degree model corresponding to our candidate model submission for SV-2010–2015 based only on CHAMP data
The extended-degree model estimated from a combination of CHAMP and Ørsted data, which was used for the uncertainty estimation of IGRF-2010 and SV-2010–2015.
The uncertainty of the two extended models is estimated in the same way as for the SV to degree 8. The higher degrees contribute very little to the overall uncertainty, which has the same RMS of 26 nT as the truncated model.
Summary of data selection criteria. Here, am and Dst are magnetic indices, IMF-By and IMF-Bz are the vector components of the interplanetary magnetic field in Geocentric Solar Magnetospheric (GSM) coordinates at the bow shock (http://omniweb.gsfc.nasa.gov/hw.html) and Em is the merging electric field (Kan and Lee, 1979). By mid latitudes we mean track segments covering −60° to 60° geomagnetic latitude and high latitudes refers to overlapping tracks at < −50° and >50° geomagnetic latitude.
Max Dst derivative
Max am 3 hours before
Max diamagnetic effect
Max jump in diam. eff.
Residuals of satellite observations against Pomme-6 and the two CHAMP-only parent models from which our candidates for IGRF-11 were derived.
Pomme-6, data range 2000.6 to 2009.67
CHAMP vector (mid-lat.)
CHAMP scalar (global)
Ørsted vector (mid-lat.)
Ørsted scalar (global)
Parent model 2005, data range 2003.5 to 2006.5
CHAMP vector (mid-lat.)
CHAMP scalar (global)
Ørsted scalar (global)
Parent model 2010, data range 2006.5 to 2009.67
CHAMP vector (mid-lat.)
CHAMP scalar (global)
Ørsted scalar (global)
4. Summary and Conclusions
Pomme-6 and three candidates for IGRF-11 have been derived from CHAMP satellite data and validated with Ørsted satellite data. All models and the software are available at our web site http://geomag.org/models/pomme6.html.
Judging from the small residuals of the data against the models, an overall accuracy of the order of 1 nT per component (at least at mid latitudes) has likely been achieved by our main field candidate for 2005. For the prediction of the main field at epoch 2010 somewhat larger and for the SV 2010–2015 much larger inaccuracies must be assumed, due to inherent problems with forecasting the future evolution of the geomagnetic field. An important question is whether the presently observed secular acceleration can be used to extrapolate the SV to the center of the upcoming epoch. Our analysis of past field behavior indicates that this is highly speculative. We have therefore taken the conservative approach of using the modeled SV at the end of the data period as an estimate of the SV for the upcoming epoch.
As an interesting secondary result, we find a systematic difference between the field strengths predicted by the CHAMP model and the Ørsted measurements at a different altitude. The Ørsted residuals appear to exhibit an additional 800 day local time periodicity. These scalar residuals show a systematic latitude variation. Peak values occur just at latitudes (~40°) where the magnetic field of the ring current does not contribute to the field magnitude. However, the discrepancy does not exhibit a behavior over time that supports the existence of a genuine difference in the ambient field strength. We are therefore not sure whether the differences are due to a deficit in external field characterization or a deviation between the scalar magnetic field readings of the two spacecraft.
We thank Brian Hamilton and Angelo DeSantis for their careful reviews and helpful suggestions. The CHAMP mission is supported by the German Aerospace Center (DLR) and the Federal Ministry of Education and Research. The Ørsted Project was made possible by extensive support from the Danish Government, NASA, ESA, CNES and DARA.
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